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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/8262
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dc.contributor.authorBhadra, Sourav-
dc.contributor.authorThoudam, Satyendra-
dc.contributor.authorNath, Biman-
dc.contributor.authorSharma, Prateek-
dc.date.accessioned2024-06-05T04:11:16Z-
dc.date.available2024-06-05T04:11:16Z-
dc.date.issued2024-02-01-
dc.identifier.citationThe Astrophysical Journal, 2024, Vol.961, p215en_US
dc.identifier.urihttp://hdl.handle.net/2289/8262-
dc.descriptionOpen Accessen_US
dc.description.abstractWe show that massive, young star clusters may be possible candidates that can accelerate Galactic cosmic rays (CRs) in the range of 107–109 GeV (between the “knee” and “ankle”). Various plausible scenarios, such as acceleration at the wind termination shock and supernova shocks inside these young star clusters, have been proposed, since it is difficult to accelerate particles up to the 107–109 GeV range in the standard paradigm of CR acceleration in supernova remnants. We consider a model for the production of different nuclei in CRs from massive stellar winds using the observed distribution of young star clusters in the Galactic plane. We present a detailed calculation of CR transport in the Galaxy, taking into account the effect of diffusion, interaction losses during propagation, and particle reacceleration by old supernova remnants to determine the all-particle CR spectrum. Using the maximum energy estimate from the Hillas criterion, we argue that a young, massive star cluster can accelerate protons up to a few tens of PeV. Upon comparison with the observed data, our model requires a CR source spectrum with an exponential cutoff of 5 × 107Z GeV (50 Z PeV) from these clusters, together with a CR injection fraction of ∼5% of the wind kinetic energy. We discuss the possibility of achieving these requirements in star clusters, as well as the associated uncertainties, in the context of considering star clusters as the natural accelerator of the “second component” of Galactic CRs.en_US
dc.language.isoenen_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2024ApJ...961..215B/abstracten_US
dc.relation.urihttps://arxiv.org/abs/2312.06992en_US
dc.relation.urihttps://doi.org/10.3847/1538-4357/ad1605en_US
dc.rights2024, The Author(s)en_US
dc.subjectCosmic raysen_US
dc.subjectParticle astrophysicsen_US
dc.subjectHigh energy astrophysicsen_US
dc.subjectGalactic cosmic raysen_US
dc.subjectYoung star clustersen_US
dc.titleBetween the Cosmic-Ray “Knee” and the “Ankle”: Contribution from Star Clustersen_US
dc.typeArticleen_US
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